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Lowson, N; Zhou, G; Huang, C X; Wright, D J; Edwards, B; Nabbie, E; Venner, A; Quinn, S N; Collins, K A; Gillen, E; Battley, M; Triaud, A; Hellier, C; Seager, S; Winn, J N; Jenkins, J M; Wohler, B; Shporer, A; Schwarz, R P; Murgas, F; Pallé, E; Anderson, D R; West, R G; Wittenmyer, R A; Bowler, B P; Horner, J; Kane, S R; Kielkopf, J; Plavchan, P; Zhang, H; Fairnington, T; Okumura, J; Mengel, M W; Addison, B C
Monthly notices of the Royal Astronomical Society, 10/2023, Letnik: 527, Številka: 1Journal Article
ABSTRACT We report the discovery of two mini-Neptunes in near 2:1 resonance orbits (P = 7.610303 d for HIP 113103 b and P = 14.245651 d for HIP 113103 c) around the adolescent K-star HIP 113103 (TIC 121490076). The planet system was first identified from the TESS mission, and was confirmed via additional photometric and spectroscopic observations, including a ∼17.5 h observation for the transits of both planets using ESA CHEOPS. We place ≤4.5 min and ≤2.5 min limits on the absence of transit timing variations over the 3 yr photometric baseline, allowing further constraints on the orbital eccentricities of the system beyond that available from the photometric transit duration alone. With a planetary radius of Rp = $1.829_{-0.067}^{+0.096}$ R⊕, HIP 113103 b resides within the radius gap, and this might provide invaluable information on the formation disparities between super-Earths and mini-Neptunes. Given the larger radius Rp = $2.40_{-0.08}^{+0.10}$ R⊕ for HIP 113103 c, and close proximity of both planets to HIP 113103, it is likely that HIP 113103 b might have lost (or is still losing) its primordial atmosphere. We therefore present simulated atmospheric transmission spectra of both planets using JWST, HST, and Twinkle. It demonstrates a potential metallicity difference (due to differences in their evolution) would be a challenge to detect if the atmospheres are in chemical equilibrium. As one of the brightest multi sub-Neptune planet systems suitable for atmosphere follow up, HIP 113103 b and HIP 113103 c could provide insight on planetary evolution for the sub-Neptune K-star population.
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